{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2009:D6YDZEKOCQVSGZSF2FIKV7HB32","short_pith_number":"pith:D6YDZEKO","schema_version":"1.0","canonical_sha256":"1fb03c914e142b236645d150aafce1de923e9a4b47115e3e59f39b8dada8ecc6","source":{"kind":"arxiv","id":"0909.1971","version":2},"attestation_state":"computed","paper":{"title":"The formation and evolution of young low-mass stars within halos with high concentration of dark matter particles","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.CO","authors_text":"Ilidio Lopes, Jordi Casanellas","submitted_at":"2009-09-10T15:19:57Z","abstract_excerpt":"The formation and evolution of low-mass stars within dense halos of dark matter (DM) leads to evolution scenarios quite different from the classical stellar evolution. As a result of our detailed numerical work, we describe these new scenarios for a range of DM densities on the host halo, a range of scattering cross sections of the DM particles considered, and for stellar masses from 0.7 to 3 M_{\\odot}. For the first time, we also computed the evolution of young low-mass stars in their Hayashi track in the pre-main sequence phase and found that, for high DM densities, these stars stop their gr"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"0909.1971","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2009-09-10T15:19:57Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"25a04eb731d6c9cd0fc471992319a484992d971f77aa9e200f8731932097336f","abstract_canon_sha256":"191a304641aae0813494fdd9b367ee4875d77ccc8d288149b9fd4c0aef27f3fc"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:34:30.553464Z","signature_b64":"FEF5qomtISW2ZLlylRxshfV+uPBTy/TbvRlL34Zv3hTxa8lRfD1b0UQsRfCpbcHwV5HOmp+rAfW1TAEjoVLTCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"1fb03c914e142b236645d150aafce1de923e9a4b47115e3e59f39b8dada8ecc6","last_reissued_at":"2026-05-18T02:34:30.552859Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:34:30.552859Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The formation and evolution of young low-mass stars within halos with high concentration of dark matter particles","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.CO","authors_text":"Ilidio Lopes, Jordi Casanellas","submitted_at":"2009-09-10T15:19:57Z","abstract_excerpt":"The formation and evolution of low-mass stars within dense halos of dark matter (DM) leads to evolution scenarios quite different from the classical stellar evolution. As a result of our detailed numerical work, we describe these new scenarios for a range of DM densities on the host halo, a range of scattering cross sections of the DM particles considered, and for stellar masses from 0.7 to 3 M_{\\odot}. For the first time, we also computed the evolution of young low-mass stars in their Hayashi track in the pre-main sequence phase and found that, for high DM densities, these stars stop their gr"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0909.1971","kind":"arxiv","version":2},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"},"aliases":[{"alias_kind":"arxiv","alias_value":"0909.1971","created_at":"2026-05-18T02:34:30.552944+00:00"},{"alias_kind":"arxiv_version","alias_value":"0909.1971v2","created_at":"2026-05-18T02:34:30.552944+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0909.1971","created_at":"2026-05-18T02:34:30.552944+00:00"},{"alias_kind":"pith_short_12","alias_value":"D6YDZEKOCQVS","created_at":"2026-05-18T12:25:59.703012+00:00"},{"alias_kind":"pith_short_16","alias_value":"D6YDZEKOCQVSGZSF","created_at":"2026-05-18T12:25:59.703012+00:00"},{"alias_kind":"pith_short_8","alias_value":"D6YDZEKO","created_at":"2026-05-18T12:25:59.703012+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/D6YDZEKOCQVSGZSF2FIKV7HB32","json":"https://pith.science/pith/D6YDZEKOCQVSGZSF2FIKV7HB32.json","graph_json":"https://pith.science/api/pith-number/D6YDZEKOCQVSGZSF2FIKV7HB32/graph.json","events_json":"https://pith.science/api/pith-number/D6YDZEKOCQVSGZSF2FIKV7HB32/events.json","paper":"https://pith.science/paper/D6YDZEKO"},"agent_actions":{"view_html":"https://pith.science/pith/D6YDZEKOCQVSGZSF2FIKV7HB32","download_json":"https://pith.science/pith/D6YDZEKOCQVSGZSF2FIKV7HB32.json","view_paper":"https://pith.science/paper/D6YDZEKO","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0909.1971&json=true","fetch_graph":"https://pith.science/api/pith-number/D6YDZEKOCQVSGZSF2FIKV7HB32/graph.json","fetch_events":"https://pith.science/api/pith-number/D6YDZEKOCQVSGZSF2FIKV7HB32/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/D6YDZEKOCQVSGZSF2FIKV7HB32/action/timestamp_anchor","attest_storage":"https://pith.science/pith/D6YDZEKOCQVSGZSF2FIKV7HB32/action/storage_attestation","attest_author":"https://pith.science/pith/D6YDZEKOCQVSGZSF2FIKV7HB32/action/author_attestation","sign_citation":"https://pith.science/pith/D6YDZEKOCQVSGZSF2FIKV7HB32/action/citation_signature","submit_replication":"https://pith.science/pith/D6YDZEKOCQVSGZSF2FIKV7HB32/action/replication_record"}},"created_at":"2026-05-18T02:34:30.552944+00:00","updated_at":"2026-05-18T02:34:30.552944+00:00"}